Results 181 to 190 of about 18,502 (219)
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From Protoplanetary to Debris Disks
2002We discuss the physical difference between protoplanetary and debris (Vega-like) disks and consider the course of evolution which leads from the first to the latter. We discuss a simple evolutionary model for debris disks and predict 20μm fluxes for future observations with VISIR.
Dominik, C., Dullemond, C.P.
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Theory of protoplanetary disks
Astrophysics and Space Science, 1995The evolution of protoplanetary disks around young stars is briefly reviewed. The most important physical mechanisms that drive the mass accretion are gravitational, magnetic, and thermal convective instabilities. These mechanisms are dominant in different regions of the disk and at different evolutionary epochs.
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Chemistry of Protoplanetary Disks
2004We consider the chemistry occurring in protoplanetary disks and its possible contribution to the organic inventory of primitive solar system bodies. First, we outline the main physical and chemical processes associated with the formation of solar-type stars and their accretion disks.
A.J. Markwickan, S.B. Charnley
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TEMPERATURES IN PROTOPLANETARY DISKS
Annual Review of Earth and Planetary Sciences, 1998▪ Abstract Observations of suspected planet-forming disks provide estimates of protoplanetary disk masses, surface temperatures, and the rate at which mass is infalling onto the disks. Analyses of primitive meteorites and comets and their components constrain the solar nebula's temperature at the locations and times where those components were formed.
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Protostellar and Protoplanetary Disks
1997It is barely a decade since the first molecular line images of disks around embedded and pre-main sequence stars were published (Beckwith et al., 1986; Mundy et al., 1986; Sargent & Beckwith 1987). In the intervening years there has been steady progress in detecting and analyzing these disks, which are an expected by-product of the star formation ...
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Protostars and Protoplanetary Disks
Astrophysics and Space Science, 1997A great wealth of observational information about young stars has been obtained at infrared and longer wavelengths in the last decade. Combined with continued theoretical progress, these observations have pushed our understanding of the overall star formation process to a satisfying level.
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